Show simple item record

Files in this item

Item metadata

dc.contributor.authorSturrock, Zoe
dc.contributor.authorHood, Alan William
dc.date.accessioned2016-09-06T12:30:08Z
dc.date.available2016-09-06T12:30:08Z
dc.date.issued2016-09
dc.identifier.citationSturrock , Z & Hood , A W 2016 , ' Sunspot rotation : II. Effects of varying the field strength and twist of an emerging flux tube ' Astronomy & Astrophysics , vol. 593 , A63 . DOI: 10.1051/0004-6361/201628360en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 242949594
dc.identifier.otherPURE UUID: d1a0aae6-c70e-4623-a41c-722f4fcdaa47
dc.identifier.otherScopus: 84988810017
dc.identifier.urihttp://hdl.handle.net/10023/9442
dc.descriptionZS acknowledges the financial support of the Carnegie Trust for Scotland. This work used the DIRAC 1, UKMHD Consortium machine at the University of St Andrews and the DiRAC Data Centric system at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk). This equipment was funded by BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1, and STFC DiRAC Operations grant ST/K003267/1 and Durham University. DiRAC is part of the National E-Infrastructure.en
dc.description.abstractContext. Observations of flux emergence indicate that rotational velocities may develop within sunspots. However, the dependence of this rotation on sub-photospheric field strength and twist remains largely unknown. Aims. We investigate the effects of varying the initial field strength and twist of an emerging sub-photospheric magnetic flux tube onthe rotation of the sunspots at the photosphere. Methods. We consider a simple model of a stratified domain with a sub-photospheric interior layer and three overlying atmospheric layers. A twisted arched flux tube is inserted in the interior and is allowed to rise into the atmosphere. To achieve this, the MHD equations are solved using the Lagrangian-remap code, Lare3d. We perform a parameter study by independently varying the sub-photospheric magnetic field strength and twist. Results. Altering the initial magnetic field strength and twist of the flux tube significantly affects the tube’s evolution and the rotational motions that develop at the photosphere. The rotation angle, vorticity, and current show a direct dependence on the initial field strength. We find that an increase in field strength increases the angle through which the fieldlines rotate, the length of the fieldlines extending into the atmosphere, and the magnetic energy transported to the atmosphere. This also affects the amount of residual twist in the interior. The length of the fieldlines is crucial as we predict the twist per unit length equilibrates to a lower value on longer fieldlines. No such direct dependence is found when we modify the twist of the magnetic field owing to the complex effect this has on the tension force acting on the tube. However, there is still a clear ordering in quantities such as the rotation angle, helicity, and free energy with higher initial twist cases being related to sunspots that rotate more rapidly, transporting more helicity and magnetic energy to the atmosphere.en
dc.format.extent15en
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© 2016, ESO, reproduced with permission. This work is made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at www.aanda.org / https://dx.doi.org/10.1051/0004-6361/201628360en
dc.subjectMagnetohydrodynamicsen
dc.subjectMethods: numericalen
dc.subjectSun: magnetic fieldsen
dc.subjectSun: interioren
dc.subjectSun: atmosphereen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleSunspot rotation : II. Effects of varying the field strength and twist of an emerging flux tubeen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201628360
dc.description.statusPeer revieweden
dc.date.embargoedUntil06-09-20


The following license files are associated with this item:

This item appears in the following Collection(s)

Show simple item record